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space_sciences/11818_50.txt | d SOT, we wanted toidentify the same feature in both instruments in order to finalize the alignment. Moreover,in addition to the intrinsic residual mis-alignment between the two instruments, the pointingof the SOT filtergraph images undergoes a drift with time due to the gross motion of solar granules seen over a narro... | |
space_sciences/25754_454.txt | brated GOES solar proton effective energies on derived integral fluxes by comparison with STEREO observations. Space Weather, 15, 290–309, doi:10.1002/2016SW001533. Singleterry Jr., R. C., Shinn, J. L., Wilson, J. W., Maiden, D. L., Thibeault, S. A., Badavi, F. F., et al. (1999). Aircraft radiation shield experiments – | |
space_sciences/05857_31.txt | e the mapping between the symbols used in a formal specification and their interpretation in the real world.
The structures that have been worked out do not apply solely to specification. In fact, they should be applied to all software lifecycle artifacts including designs and implementations. The reason is that all a... | |
space_sciences/07274_49.txt | t wavelength infrared (SWIR) and MWIR spectral range.
III-V Compound Material Systems
QWIP based on III-V compound materials have been extensively investigated for high background using large area highly uniform focal plane arrays (FPAs) and this technology demonstrates considerable development in the fabrication of ... | |
space_sciences/15884_96.txt | medspectrum into at least 1 count per bin using Cash statistics toperform the spectral fit.
We fitted the spectrum of this point source with severalmodels: simple PL, a thermal plasma (APEC) plus a PL,and a multi-color accretion disk (MCD) with a PL. Table 5lists the best-fitting parameters and the observed soft and ha... | |
space_sciences/09386_120.txt | s are generally too small for detection from Earth, but can be observed from the inner heliosphere.
By traveling close to the Sun with remotesensing and in-situ measurements, Sentinels and Solar Orbiter will revolutionize our understanding of SEPs. The mixing effects, so dominant at Earth orbit, will be largely remove... | |
space_sciences/13448_19.txt |
2.1. Discovery of a CRSF in 1A 1118+61
After only two previously observed outbursts (1974, 1992) the Be X-ray binary lA 1118-61 went into outburst in January 2009 and was observed with Suzaku at the rv 500 mCrab outburst peak and two weeks later at the end of the main outburst (Fig. 1, left) | |
space_sciences/20350_107.txt | e quite unlikely to be members of the background variation in reflectance due to ordinary lunar geologic processes. We identify those areas by first computing the statistics of the reflectance distribution of polar areas with maximum temperatures too warm to support the presence of surface ice. We then compare the refl... | |
space_sciences/06926_97.txt | bution, but is probably not significant between 2.2 pm and 2.0 pm. Other factors besides grain length and width contribute to q, such as efficiency of grain alignment as a function of grain size, grain size distribution, and magnetic field orientation with respect to the plane of the sky (Jones et al. 1992); consequent... | |
space_sciences/17871_77.txt | IAA-2010-6294, 2010. 6. Ticker, R., “Engineering Test Beds on the International Space Station”, IEEE A&E Systems Magazine, August 2009.7. Swanson, T.D., Birur, G. C., “NASA Thermal Control Technologies for Robotic Spacecraft”, National Aeronautics and Space Administration, N20030031332, 2003.8. Westheimer, D. T., Tuan,... | |
space_sciences/07710_6.txt | rbes Avenue, Pittsbwqh, PA 15213, USA ' Department of Physics, Uniuersity of Durham, South Road, Durham, DHl 3LE, UK lo Departmmt of Physics, Nagoya University, EIUro-cho, Chikusa, Nagoya 464-8602 Department of Physics, Tokyo Institute of Tahriology, 2-12-1, Meg | |
space_sciences/17161_19.txt | D,28 QUIJOTE,29BICEP3,30 PIPER31 and CLASS.32 In March 2014 the BICEP2 team,33 claimed a detection of primordial Bmodes consistent with a tensor-to-scalar ratio r of 0.2, in tension with r < 0.1134 upper limit from temperatureanisotropy measurements. Confirmation of this claim requires better understanding of the polar... | |
space_sciences/15149_57.txt | l outbursts in 2009 August and 2010 July (see Figure 2). Wepoint out that the one in 2009 August showed two approximatelyequal peaks in both duration and intensity (see the left panel ofFigure 2) without the typical shape of pre-periastron peaks described before. The last peculiar outburst in 2010 July was onlyentirely... | |
space_sciences/09224_69.txt | s, which do not require the continuous treatment of the free-stream to postshock transition.
The influences of both coupled ablation and radiation on the stagnation-line temperature and wall-directed radiative flux profiles are shown in Figures 7 and 8. Significant decreases in the temperature and radiative flux profi... | |
space_sciences/16702_5.txt | Gullstrand form of the metric of the Schwarzschild black hole [2, 3]. This metric has attracted renewed interest of late, due to its useful properties, which include thefollowing: (i) its hypersurfaces of constant time are flat; (ii) its coordinates are well-behavedat the horizon; (iii) its time coordinate (which is ti... | |
space_sciences/00980_28.txt | s. Encryption, digital signatures, and otherdata security measures can be used to protect proprietary data.
2.3 Cost Savings via Ground Automation
A Nexus requirement for ground system automation did not result in significant savings. The broadly statedrequirement was at odds with the objectives of low cost development... | |
space_sciences/24649_69.txt | n to the tablets, whichran the preloaded application throughout the test series (Figure 23). However, the effects of water pressure andcapacitance saturated the touch screen, making all attempted touch command interfaces unusable. These results havedelayed the availability of the interactive underwater control stations... | |
space_sciences/03147_41.txt | T HR2 of X23 and lack of time variabilitymay point to it being a SNR.
While a detailed spectral and time variability studyof all the NGC 253 sources is beyond the scope of the
present paper, we demonstrate here the capabilities of theEPIC instrument on the brightest point source, X33. Itsspectrum (Fig. 2) can be fit by... | |
space_sciences/13290_101.txt | t is not surprising that highest priority is placed on the precise determination of Apophis' state vector. The second priority of the mission is determination of the composition of Apophis in terms of mineralogy and any potential presence of organic materials. 7.2.c. Candidate Architecture Definitions
The next step in... | |
space_sciences/15221_116.txt | .911, O II/O = 0.077 and O III/O = 0.012. Regardingthe oxygen abundance, it may be clarified that the quoted value is given relative tothe solar standard (8.83 ± 0.06) of Grevesse & Sauval (1998). If it is rescaled to therecently revised standard by Asplund et al. (2009) of 8.69 ± 0.05, then an ISM abundance | |
space_sciences/18985_104.txt | e from flux, delta-t do j = 1,34 flue(j) = flue(j) + (et - etold) * dble(flux(j)) enddo etold = et go to 1 2001 continue ictold = n print*,'orbit ends at line ',ictold C write output file line2 = ' Fluences estimated by use of a pre-caclulated grid of po +ints using | |
space_sciences/11542_26.txt | n and statetransitions consistent with the current observational scenario of classical accreting BH inoutburst. Specifically, XTE J1752-223 went through the initial LHS, transitioned throughIS to HSS, returned to LHS and decayed to quiescence. The very high state, sometimescalled the steep power law state (Remillard & ... | |
space_sciences/09518_169.txt | , M. Meyer (Steward).
References
1. Albrecht A,, et al. 2006, DETF report, http://home.fnal.gov/iocky/DETF/; 2. Amendola, L., 2000, Phys.Rev. D, 62, 3511 ; 3. Angulo R., et al. 2005, MNRAS, 362. L25 ; 4. Angulo R., et | |
space_sciences/07354_27.txt | 793Wu, C.Y.R., Judge, D.L., Cheng, B. -M., Lee, C.S., Yih, T.S., & Ip, W. H. 2003, J. Geophys.Res, 108(E4), 5032Wu, C.Y.R., Judge, D.L., Cheng, B. -M., Chih, Yih, T.S., & Ip, W. H. 2002, Icarus, | |
space_sciences/04049_40.txt | h are (d) 6, (e) 12, and (f) 18. Now diffusion is dominant on the day side while drift is dominant on the night side, as can be seen from the MLT (magnetic local time) labels in each case. In the first two (d and e) the DLC region to the east of the SAA (0 to 90' dipole longitude) is on the dayside and is filled in by ... | |
space_sciences/01394_51.txt | 2344+514)and the fourth, Mrk 421, is somewhere in the middle.Blue blazars are less luminous (Fossati et al. 1998),which may result from differences in outflow Lorentzfactors (Kubo et al. 1998). The particle accelerationprocess in blazars is not known and neither is how they"cool their jets," that is, how the environme... | |
space_sciences/16501_36.txt | t source amplitudes,and the SZ amplitude (Keisler et al. 2011). For ACT we usethe 148 GHz power spectrum from Das et al. (2011b) in themultipole range 500 <l< 10000, marginalizing over thesame clustered point source and SZ amplitudes as in the SPTlikelihood, but over a separate Poisson source amplitude. SeeSections 2.3... | |
space_sciences/11262_29.txt | mulated and limit switches (not shown in models) are used to reliably detect proximity of hard stops. The limit switches in conjunction with hard-stops are approximately 360° apart and allow for the angular position at the respective extremes to be known by the MCU. One of the limit-switch/hard-stops will be designated... | |
space_sciences/13568_476.txt | ⊕ and P=2 yrs is ~0.5%, and thus ~100/0.005 = 2x104 microlensing events must be monitored to detect ~100 such planets. The microlensing event rate in the highest density fields accessible by WFIRST is ~2×10-5events/year, and thus 2x104/2×10-5~1 billion star-yearsmust be monitored. The typical stellar density down to J=... | |
space_sciences/10031_52.txt | r could fhrrll. Ni~lsei~ et ill. (2007ii.) traced. \$-it11 HSTiS'YIS spectra. Hr I lines forlncti ill
t~~de tlle wintl-wind iliterfiice over tllr 5.53 year spectroscopic period to fi1rt1lc.r anill)-ze tllr io~iizatioil structure of thc n-it~tl and cl~ | |
space_sciences/03526_88.txt | , M.M., Lallement, R, 1999, A&A, Yoshioka, S., Ikeuchi, S., 1990, Ap. 3. 360, 352 and A.C. Fabian (Cambridge University Press), 240 Astrophys. 389, 93L Instrumentation for Astronomy IV, 2006, 221 and Morgenthaler, J.P., 2001, Ap.J. 554, 694 sky P.P. | |
space_sciences/09637_55.txt | . T. Schweizer, these proceedings.
18. S. A. Story, P. L. Gonthier, A. K. Harding, ApJ 671,713-726 (2007).19. M. Tavani et al., Nucl. Inst. Meth. A 588, 52-62 (2008).20. M. Teshima., Astron. Tel. 1491, (2008).21. D. J | |
space_sciences/16191_71.txt | −4532 is∼13 kpc (Rahoui et al. 2008).
During the eclipse of IGR J16418−4532, we detect a non-zeroflux with the XRT (LX ∼ 3 × 1034 erg s−1; see Fig. 4). Detectionsof HMXBs during the eclipse are quite common (see e.g. Clark,Minato & Mi 1988; Sako et al. | |
space_sciences/25539_50.txt | n/Velocity/Time (PVT) navigation solutions to replace less timely orbit estimatesfrom the ground. This constitutes the only a-priori information needed, i.e. to initialize, each observer must possess a coarse estimate of its own orbit at a single epoch. | |
space_sciences/07695_5.txt | s far too low for liquid water [2]. Many organic compounds have been detected in Titan’s atmosphere. These form as a result of the recombination of molecular fragments produced by methane (and nitrogen) photolysis. Ultraviolet solar radiation is primarily responsible, although irradiation by electrons in Saturn’s magne... | |
space_sciences/18034_86.txt | a joint likelihood analysis of multipleHVCs may provide a sensitive test of dark matter annihilation.
We note that during the final preparation of this paper, Nicholset al. (2014) reported upper limits on the dark matter annihilationcross section from Fermi-LAT observations of the Smith Cloud.While our results are qual... | |
space_sciences/06984_29.txt | vatory and Royal Observatory of Belgium sunspot number values against Rome Observatory determinations of sunspot number. Previously, it has been shown that both sunspot area and sunumber, as determined today, appear slightly different (underestimated and overestimated, respectifrom earlier years when sunspot areas were... | |
space_sciences/23592_101.txt | c1aa5576 0x000221cf.pdf 13, 17–21.
Benson, J., Freeman, J. W., Hills, H. K., 1975. The lunar terminator ionosphere. Lunar and Planetary Science Conference Proceedings 3, 3013–3021.
Catling, D. C., Kasting, J. F., 2017. Atmospheric Evolution on Inhabited andLifeless Worlds. Cambridge University Press, New York. | |
space_sciences/20817_1.txt | Numerical simulation of illumination and thermal conditions at thelunar poles using LOLA DTMs
P. Gläser1, D. Gläser2, J. Oberst1,3, G.A. Neumann4, E. Mazarico4, M.A. Siegler51Technische Universität Berlin, Institute of Geodesy and Geoinformation Science, Straße des 17. Juni 135, 10623 Berlin²University of Stuttgart, De... | |
space_sciences/00604_387.txt | - 33rd COSPAR General Assembly,paper PSRBI-O002, 2000.
244. Steenberg, C. D., A. C. Cummings, and E. C. Stone, Modeling anomalouscosmic ray composition and charge state during solar minimum, Adv.Space Res. - 33rd COSPAR General Assembly, paper D1.1-0006, 2000.
245. Baker, D. N., C. A. Barth, K. Mank | |
space_sciences/23742_168.txt | peline is applied to the real BK15X data.
4 Implications for instrument design and calibration
The requirements on the bandpass and polarization angles in table 2 have several implications both for the instrument design and the calibration plan for SO and future CMBexperiments. In this section, we discuss how these req... | |
space_sciences/22664_17.txt | e equator, not at the poles [10], [11], [12], [13]. The variation of reentry locations, especially around an ellipsoidal Earth, implies that the entry conditions will also differ: speed relative to the atmosphere and flight path angle (FPA) both change as a function of argument of latitude; see Fig. 2 for a geometric d... | |
space_sciences/01050_45.txt | sling et al., 1998].
Several processes can contribute to the expansion of a CME. A CME can expand simplybecause it is injected into the solar wind with a substantial front-to-rear speed gradient. Anotherpossibility is that expansion is a CME’s response to a rarefaction wave produced by relativemotion between the CME an... | |
space_sciences/24942_74.txt | s Earth-facing disk passage. Accordingto the Hinode Flare Catalog (Watanabe et al. 2012), however,all but one of these flares (26/27), occurred prior to the EISobservations on November 10, so any impact on thecompositional structure of AR 12781 between the EIS andSPICE observations was likely to have been minimal. Figu... |
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